| Autor: |
McLeod AF; School of Physical and Chemical Sciences, University of Canterbury, Christchurch, New Zealand., Reiter M; Department of Astronomy, University of Michigan, Ann Arbor, Michigan, USA., Kuiper R; Institute of Astronomy and Astrophysics, University of Tübingen, Tübingen, Germany., Klaassen PD; UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK., Evans CJ; UK Astronomy Technology Centre, Royal Observatory Edinburgh, Edinburgh, UK. |
| Abstrakt: |
Highly collimated parsec-scale jets, which are generally linked to the presence of an accretion disk, are commonly observed in low-mass young stellar objects. In the past two decades, a few of these jets have been directly (or indirectly) observed from higher-mass (larger than eight solar masses) young stellar objects, adding to the growing evidence that disk-mediated accretion also occurs in high-mass stars, the formation mechanism of which is still poorly understood. Of the observed jets from massive young stars, none is in the optical regime (massive young stars are typically highly obscured by their natal material), and none is found outside of the Milky Way. Here we report observations of HH 1177, an optical ionized jet that originates from a massive young stellar object located in the Large Magellanic Cloud. The jet is highly collimated over its entire measured length of at least ten parsecs and has a bipolar geometry. The presence of a jet indicates ongoing, disk-mediated accretion and, together with the high degree of collimation, implies that this system is probably formed through a scaled-up version of the formation mechanism of low-mass stars. We conclude that the physics that govern jet launching and collimation is independent of stellar mass. |
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